Remnant baryon mass outside of the black hole after a neutron star-black hole merger
read the original abstract
Gravitational-wave (GW) and electromagnetic (EM) signals from the merger of a Neutron Star (NS) and a Black Hole (BH) are a highly anticipated discovery in extreme gravity, nuclear-, and astrophysics. We develop a simple formula that distinguishes between merger outcomes and predicts the post-merger remnant mass, validated with 75 simulations. Our formula improves on existing results by describing critical unexplored regimes: comparable masses and higher BH spins. These are important to differentiate NSNS from NSBH mergers, and to infer source physics from EM signals.
This paper has not been read by Pith yet.
Forward citations
Cited by 3 Pith papers
-
Gravitational wave detectability range informed by external messengers
The Targeted Detectability Range (TDR) incorporates sky localization, inclination constraints, and mass bounds from external messengers to evaluate gravitational-wave detectability for gamma-ray bursts observed during...
-
Massquerade: Impacts of Mass Ratio Reversals on Binary Black Hole Merger Rates and Mass Distributions
Mass ratio reversals produce qualitatively different contributions to BBH merger rates and masses in COMPAS versus SEVN simulations, with core-growth dominating and most systems arising from massive low-metallicity pr...
-
Alfven-winged pulsar
A neutron star in a compact binary generates relativistic Alfven wings that carry most of the intersected electromagnetic power and may produce periodic pulsar-like emission.
discussion (0)
Sign in with ORCID, Apple, or X to comment. Anyone can read and Pith papers without signing in.